Solar neutrino emission deduced from a seismic model

Three helioseismic instruments on the Solar and Heliospheric Observatory ha ve observed the Sun almost continuously since early 1996. This has led to d etailed study of the biases induced by the instruments that measure intensi ty or Doppler velocity variation. Photospheric turbulence hardly influences the tiny signature of conditions in the energy-generating core in the low- order modes, which are therefore very informative. We use sound-speed and d ensity profiles inferred from GOLF and MDI data including these modes, toge ther with recent improvements to stellar model computations, to build a sph erically symmetric seismically adjusted model in agreement with the observa tions. The model is in hydrostatic and thermal balance and produces the pre sent observed luminosity. In constructing the model, we adopt the best phys ics available, although we adjust some fundamental ingredients, well within the commonly estimated errors, such as the p-p reaction rate (+1%) and the heavy-element abundance (+3.5%); we also examine the sensitivity of the de nsity profile to the nuclear reaction rates. Then, we deduce the correspond ing emitted neutrino fluxes and consequently demonstrate that it is unlikel y that the deficit of the neutrino fluxes measured on Earth can be explaine d by a spherically symmetric classical model without neutrino flavor transi tions. Finally, we discuss the limitations of our results and future develo pments.